Abstract

Entry Probe Missions to the Giant Planets

The primary motivation for in situ probe missions to the outer planets derives from the need to constrain models of solar system formation and the origin and evolution of atmospheres, to provide a basis for comparative studies of the gas and ice giants, and to provide a valuable link to extrasolar planetary systems. The gas and ice giants offer a laboratory for studying the atmospheric chemistries, dynamics, and interiors of all the planets, including Earth, for it is within the deep, well-mixed atmospheres and interiors of the giant planets that pristine material from the epoch of solar system formation can be found, providing clues to the local chemical and physical conditions existing at the time and location at which each planet formed. Although planetary entry probes sample only a small portion of a giant planet’s atmosphere, probes provide data on critical properties of atmospheres that cannot be obtained by remote sensing, such as measurements of constituents that are spectrally inactive, constituents found primarily below the visible clouds, and chemical, physical, and dynamical properties at much higher vertical resolutions than can be obtained remotely. The Galileo probe, for instance, returned compositional data at Jupiter that has challenged existing models of Jupiter’s formation. To complement the Galileo in situ explorations of Jupiter, an entry probe mission to Saturn is needed.  To provide for comparative studies of the gas giants and the ice giants, additional probe missions to either Uranus or Neptune are essential.

Come meet the speaker over coffee and refreshments from 3:45-4:10 pm in the foyer on floor G above the lecture hall.   All Welcome.  Host: Chuanwei Zhang